All Figures

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8cm,clip]{7040fig1.eps} \includegraphics[angle=-90,width=8cm,clip]{7040fig2.eps} } \end{figure}$ Figure 1: The Aitoff projection in galactic coordinates of all the WFC observation pointing directions ( left) and of the FOV of a typical WFC pointing of the Galactic Center (the circle includes the squared WFC FOV). WFC unit 1 points at Sgr-A and unit 2 at the anti-center, including the Crab Nebula.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7040fig3.eps}\par\includegraphics[width=8cm,clip]{7040fig4.eps}\end{figure}$ Figure 2: The 2-10 keV Crab Nebula ( top panel) and Cas A secular light curves corrected for the linear decrease with off-axis angle described in the text (open circles correspond to unit 1). A systematic error of $\sim$ 2% was added in quadrature to the corrected flux errors for both WFCs to reach a reduced chi-square of $\sim$ 1. Residual dispersions for corrected light curves are 2% and 6.2% respectively.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm,clip]{7040fig5CMJN.eps} \includegraphics[width=8cm,clip]{7040fig6.eps} } \end{figure}$ Figure 3: The cumulative 2-8 keV SNR distributions of all the detections without any SNR cut for the first data processing run ( left panel) and for the most complete one. The upper black thick curves are the total samples, the dash-dotted curves are the components of the fitted models (Gaussian + Broken power law, with parameters mean = 3.9, $\sigma =1.2$ , slopes $\sim$ -0.53 and $\sim$ -0.01 and break at $\sim$ 4.0 for the first processing run and mean = 4.0, $\sigma$ = 1.2, same slopes and break at $\sim$ 5.8), while the remaining three lower curves are the distributions for different off-axis angle intervals (the circled one corresponds to off-axis angles <10 $^\circ$ , the squared to 10-15 $^\circ$ and the triangled to >15 $^\circ$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7040fig7CMJN.eps}\end{figure}$ Figure 4: The cumulative distributions of SNR in three larger/harder bands (2-26, 8-19, 19-26 keV) for detections of the second processing run. The Gaussian component of the model fitted to the 8-19 keV curve is shown.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7040fig8CMJN.eps}\end{figure}$ Figure 5: The Aitoff projection of the BeppoSAX WFC detections: 8283 detections of 253 distinct X-ray sources in all the observations processed (symbol size is proportional to intensity).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7040fig9.eps}\end{figure}$ Figure 6: The exposure distributions of the BeppoSAX WFC detections in all data processed.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7040fig10.eps}\par\includegraphics[width=8cm,clip]{7040fig11.eps}\end{figure}$ Figure 7: The 2-10 keV flux as a function of the exposure ( top panel) of the final sample of detections. The dashed lines on the bottom part of the plot show the limiting sensitivity model (proportional to the exposure square root) for fields out of the Galactic Plane ( the lowest) and the GC ones. In the bottom panel the same flux vs the off-axis angle. The dashed curve on the bottom part of the plot shows a model of the limiting sensitivity as a function of the off-axis angle.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7040fig12.eps}\par\includegraphics[angle=-90,width=8cm,clip]{7040fig13.ps}\end{figure}$ Figure 8: Positional 99% error radius (in arcmin) as a function of the SNR ( top panel), where each data point represents the average over 150 source positions and the standard deviation with respect to that average. In the bottom panel the cumulative distribution of the distances between measured positions and those in the reference catalogue (in arcminutes) for all the detections (upper curve) and for detections with ${\it SNR}>60$ and ${\it SNR}>180$ . The radii including 99% of the detections are $\sim$ 3.3 $^\prime$ , 1.87 $^\prime$ and 1.78 $^\prime$ respectively. The dashed curve is the cumulative Gaussian component of the fit model applied to the upper curve, which represent the expected model for bright sources.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7040fig14.ps} % \end{figure}$ Figure 9: The positions of all Cyg X-1 detections in equatorial coordinates. Crosses correspond to WFC unit 1, circles to unit 2, while the star corresponds to the Cyg X-1 reference catalogue position, RA = 299.5904, Dec = 35.2016 and the encircled cross to the best fit position, RA = 99.5898, Dec = 35.2021. The thick circle of radius $\sim$ 1.6 $^\prime$ represents the 95% confidence level centered on the Gaussian model best fit position.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7040fig15.ps} \end{figure}$ Figure 10: Spurious matches in the cross-correlation of the BeppoSAX WFC catalogue with the reference catalogue with a radius of 5 $^\prime$ for "shift'' values from 0 $^\circ$ to 2 $^\circ$ .
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm,clip]{NEW7040fig16.ps}\hspace{0.7cm} \includegraphics[width=8cm,clip]{7040fig17.ps} } \end{figure}$ Figure 11: The Hardness Ratio 1 (1.7-3.2/4.6-7.1 keV bands; left panel) distributions for each source class included in the catalogue. On the right the same per classes distributions of Hardness Ratio 2 (4.6-7.1/7.1-10.9 keV). Two corresponding energy indexes, evaluated assuming galactic absorption, are shown in the top scales of both panels. Numbers below each class label, in both panels, are the detections having non-null values of count rates and of energy indexes.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8cm,clip]{7040fig1.eps} \includegraphics[angle=-90,width=8cm,clip]{7040fig2.eps} } \end{figure}$	Figure 1: The Aitoff projection in galactic coordinates of all the WFC observation pointing directions ( left) and of the FOV of a typical WFC pointing of the Galactic Center (the circle includes the squared WFC FOV). WFC unit 1 points at Sgr-A and unit 2 at the anti-center, including the Crab Nebula.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7040fig7CMJN.eps}\end{figure}$	Figure 4: The cumulative distributions of SNR in three larger/harder bands (2-26, 8-19, 19-26 keV) for detections of the second processing run. The Gaussian component of the model fitted to the 8-19 keV curve is shown.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7040fig8CMJN.eps}\end{figure}$	Figure 5: The Aitoff projection of the BeppoSAX WFC detections: 8283 detections of 253 distinct X-ray sources in all the observations processed (symbol size is proportional to intensity).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7040fig9.eps}\end{figure}$	Figure 6: The exposure distributions of the BeppoSAX WFC detections in all data processed.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7040fig15.ps} \end{figure}$	Figure 10: Spurious matches in the cross-correlation of the BeppoSAX WFC catalogue with the reference catalogue with a radius of 5 $^\prime$ for "shift'' values from 0 $^\circ$ to 2 $^\circ$ .
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